12 note(s) found in NED.

Re:NGC 2683
According to Merrifield & Kuijken (1999), the PV diagram of
NGC 2683 has a "figure-of-eight'' shape produced by the
presence of two kinematically distinct gaseous components.
This feature is barely visible in our PV diagram because of
the lower S/N ratio of the spectrum. Although the properties
of the PV diagram of NGC 2683 are similar to those of NGC 980,
NGC 2179 and NGC 7782, it does not warrant a Type I
classification. Indeed in NGC 2683 we are observing two gas
components which are spatially distinct and superimposed
along the line of sight because of the high inclination of
the galaxy (i = 78^deg^). They are generated by the presence
of a non-axisymmetric potential (Kuijken & Merrifield 1995;
Bureau & Athanassoula 1999).
This is not the case for NGC 980, NGC 2179 and NGC 7782,
which are less inclined (i = 58^deg^, 47^deg^ and 58^deg^,
respectively) and unbarred, exhibiting unique gaseous
components.

Re:NGC 2683
NGC 2683: The complex kinematics of this galaxy has been unveiled by
Pompei & Terndrup (1999) who isolated two kinematically distinct gaseous
components giving rise to a "figure-of-eight" velocity curve. The fast and
the slow-rotating components are unresolved in our spectrum as well as in
that of Barbon & Capaccioli (1975). We therefore measured intermediate
V_g_'s and higher {sigma}_g_'s.

Re:NGC 2683
NGC 2683: The H I position-velocity diagram by Broeils & van Woerden (1994)
shows two kinematically distinct components giving a "figure-of-eight"
appearance to the diagram. These components may be associated with the fast
and slow-rotating components observed by Pompei & Terndrup (1998) both in
the stellar and ionized-gas velocity curves. Figure-of-eight velocity
curves have been explained by Kuijken & Merrifield (1995) to be due to the
presence of a bar (see other examples in Vega Beltran et al. 1997;
Bureau & Freeman 1999).

Re:NGC 2683
NGC 2683 has an unresolved radio core and weak emission toward the
north-northeast. The FIRST (Faint Images of the Radio Sky at Twenty cm)
Survey image also shows a core and a second component approximately 11"
from the nucleus, which agrees in position with the strongest northeast
component in our map. A small very bright optical nucleus is also
observed (NED), the galaxy has been classified as having a
low-ionization region nucleus (Keel 1983), and X-ray emission is also
observed from its central region (Fabbiano et al. 1992). On these
grounds, this galaxy could be a candidate for a previously unknown AGN.
However, the luminosity of the radio core is low (Table 3) and could be
accounted for alternatively by a single supernova remnant. Previous
lower resolution 20 cm images can be seen in Paper I and Gioia &
Fabbiano (1987). A FIR image can be seen in Alton, Davies, & Trewhella
(1998). This is also one of the two galaxies presented by Casertano &
van Gorkom (1991) as having a declining rotation curve.

Re:NGC 2683
3.2 NGC 2683 = UGC 4641 = PGC 24930 = IRAS 08493+3336
A view of this Sb-type galaxy is shown in a mosaic (Fig. 3) constructed
from three frames in the R filter with 30 s exposure each. Figure 4
presents images of the northern (a) and southern (b) parts of the galaxy
in the V band after subtracting the frames smoothed with a median filter
with a 10x FWHM window. As one can see from these images, the whole body
of the galaxy is spotted with dusty lines, which impedes accurate
photometry of stars, especially in the B band. The results of our
photometry of 327 stars and star-like objects are presented in the
diagram V proportional to V - I (Fig. 5). The stars from the northern
galaxy side are indicated by dark circles, and the southern part stars
are marked by open boxes. A considerable part of the brightest blue
objects have a diffuse or elongated shape. After removing them we
selected three stars as blue supergiant candidates. Their mean apparent
magnitude, 20.64, yields a distance modulus of 29.81 with A_B_ = 0.07.
Note that the the brightest red (B-V > 1.6) stars in the galaxy have
V = 22.0, which corresponds to a distance modulus of about 30.0 that
agrees with the "blue" modulus. According to Tully (1988) NGC 2683 is
situated in the scattered cloud "Leo spur", which probably moves with a
peculiar velocity of about -200 km s^-1^ with respect to the Local
"pancake". This can explain the low radial velocity of the galaxy,
V_0_ = 364 km s^-1^, at its rather large distance of 9.2 Mpc. From
Karachentseva & Karachentsev (1998) and Huchtmeier et al. (2000) there
are two dwarf companions in the vicinity of NGC 2683: kk69 with
V_h_ = 420 km s^-1^ and the dwarf spheroidal system kk70. The rotation
curve for NGC 2683 was studied in the H I line by Broeils & van Woerden
(1994).

Re:NGC 2683
NGC 3521 and 2683.--These are given by Casertano & van Gorkom (1991) as
examples of galaxies with declining rotation curves. The contribution of the
gas to the Newtonian rotation curve is not shown here because the mean radial
distribution of the gas is not given in this reference; in any case, the total
gas mass, estimated from global 21 cm line profiles (Table 1), is less than
10% of the fitted disk mass (Table 3) in both cases. The photometry by Kent
(1985) includes decompositions into exponential disks and r^1/4^ law bulges.
Here the models, rather than the detailed light distributions, are used to
determine the Newtonian rotation curves. The observed rotation curves are not
ideal for estimating the true run of circular velocity. In neither case is the
rotation curve determined from a full two-dimensional radial velocity field.
In NGC 3521, the distribution of H I is asymmetric, extending 20% farther on
one side than on the other, and the velocity structure is asymmetric; NGC 2683
is nearly edge-on. Thus these galaxies fail in several respects to satisfy the
selection criteria of BBS. Nonetheless, the rotation-curve fits demonstrate
that MOND is quite capable of reproducing declining rotation curves if the
mass distribution is sufficiently centrally concentrated, a point made by
Milgrom in his original paper (Milgrom 1983). In NGC 3521, the abrupt decline
in rotational velocity between 20 and 28 kpc could he, if confirmed,
problematic for MOND, although it would also be problematic for Newtonian
dynamics since the decline is steeper than Keplerian.

Re:NGC 2683
Sb(nearly on edge)
PH-7706-S
Feb 11/12, 1980
103aO
12 min
The large angular diameter of the main disk
of NGC 2683 is 7'. A principal feature is the
X-shaped halo (well seen on the original plate).
The nucleus is small and is only seen above the
center; the lower part is blocked by the heavy
dust in the near side of the disk. The spiral
pattern is of the MAS type (multiple arms),
defined principally by the dust. Faint outer arms
exist. HII regions are present, strung along the
outer arm that is down and to the right in the
orientation of the print here.
The redshift of NGC 2683 is unexpectedly
low at v_o = 399 km/s, considering the poor
resolution of the stellar content even in the outer
arms.